From a dynamical point of view, it would be an unproblematic configuration, since both planets maintain a sufficient spatial separation to preserve long-term stability.
In addition, the longer-period planet candidate, whose expected bulk mass would require a significant gaseous envelope, is far enough from the star to avoid significant atmospheric losses due to photoevaporation [1]}.
A Neptunian-mass planet at this orbit is, thus, plausible.
In fact, core accretion theory, which is considered the most promising path of planet formation, routinely predicts planets like those found in TOI-1201.
Global formation models of multi-planetary systems [2]} find the tentative two-planet configuration to be a rather typical outcome [3]}.
New planetary population syntheses specifically tailored to M-dwarf systems also propose the regular formation of planets in the mass range of TOI-1201 b and the tentative TOI-1201 [c] [4]}.
Therefore, we believe that the latter is a promising candidate planetary companion. Further observations, especially with longer ground-based coverage, will be necessary to unequivocally determine the nature of the signal.
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